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Eddington luminosity
Mass – Luminosity Relation for Massive Stars
Testing Quantum Gravity with LIGO and VIRGO
Astronomy 112: the Physics of Stars Class 10 Notes: Applications and Extensions of Polytropes in the Last Class We Saw That Poly
Ultraluminous X-Ray Pulsars
Exceeding the Eddington Limit
A Supercomputer Models a Blinking, Impossibly Bright 'Monster Pulsar' 8 September 2016
Models of Hydrostatic Magnetar Atmospheres at High Luminosities
Luminous Blue Variables & Mass Loss Near the Eddington Limit
Supermassive Mass Black Holes
Modified Theories and Non-Singular Black Holes
© in This Web Service Cambridge University
Arxiv:1807.06243V1 [Astro-Ph.HE] 17 Jul 2018
Luminosity, Selfgravitation and Nonuniqueness of Stationary Accretion
Levitating Atmospheres of Eddington-Luminosity Neutron Stars
Massive Pulsars and Ultraluminous X-Ray Sources
Arxiv:1904.05363V3 [Gr-Qc] 13 Jun 2019
Convection 21 September 2011
BIFURCATION in the SHAKURA MODEL∗ Krzysztof Roszkowski
Top View
Inaugural Dissertation
Eddington Capture Sphere Around Luminous Stars
Download This Article in PDF Format
Ultraluminous X-Ray Pulsar: Accreting Magnetar?
5 Accretion Flows
Accreting, Highly Magnetized Neutron Stars at the Eddington Limit: a Study of the 2016 Outburst of SMC X-3 Filippos Koliopanos1,2 and Georgios Vasilopoulos3
Arxiv: Testing the Nature of Dark Compact Objects: a Status Report
Cosmology and Extragalactic Astronomy Black Holes Part II
Can Accretion Disk Properties Distinguish Gravastars from Black
Lecture 7 Evolution of Massive Stars on the Main Sequence and During
Black Holes Physics
Distinguishing Brans–Dicke–Kerr Type Naked Singularities and Black Holes with Their Thin Disk Electromagnetic Radiation Properties
Super-Eddington Accretion Onto Black Holes and Neutron Stars
Testing the Nature of Dark Compact Objects: a Status Report
Instability & Mass Loss Near the Eddington Limit
Stellar Disruption Events Support the Existence of the Black Hole Event Horizon
Astronomy 112: the Physics of Stars Class 14 Notes: the Main
Introduction Exercise 1
Core Collapse Supernovae Our Topic Today Is the Post-Main Sequence
On the Maximum Accretion Luminosity of Magnetized Neutron Stars
1 Eddington Luminosity Or Eddington Limit Ilya Mandel Ilya.Mandel
The Role of Black Holes in Galaxy Evolution Black Hole Phenomenology
The Sub-Eddington Boundary for the Quasar Mass–Luminosity Plane: a Theoretical Perspective
An Accreting Low Magnetic Field Magnetar for the Ultraluminous X
Stellar Mass Black Holes and Ultraluminous X-Ray Sources
Massive Main-Sequence Stars Evolving at the Eddington Limit⋆
The Eddington Limit
Space Exploration & Space Colonization Handbook
Physics an Overview
Eta Carinae and the Luminous Blue Variables 3 Are Thus Whether “Η Car Is Unique Among the Lbvs?” and “What Is the Root Cause of the S Doradus Variations?”
Phenomenological Aspects of Black Holes Beyond General Relativity
Mass Loss of Massive Stars Near the Eddington Luminosity by Core Neutrino Emission Shortly Before Their Explosion
Thesis Was Carried out at the University of Amsterdam, with financial Support from the European Research Council
How Do We Know What We See Is a Black Hole? Bogusz Kinasiewicz Marian Smoluchowski Institute of Physics Jagellonian University, Cracow, Poland